[ITAL]BV[/ITAL] Photometry of the RR Lyrae Variables of the Globular Cluster M3

Corwin, T. M.; Carney, Bruce W.

doi:10.1086/323918

Cited by 78 publications

(111 citation statements)

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“…We suggest instead that many of these stars are more likely to be ''blue loop stars.'' Also in passing, we note that the RRL stars that have been found ''below the ZAHB'' in M3 (Corwin & Carney 2001; see also Jurcsik 2003) may simply be a consequence of an imperfect analogy between zero-age main sequence (MS), on the one hand-a line very close to which low-mass MS stars will indeed spend most of their MS lifetimes-and ZAHB, on the other-the ZAHB not being, in general, a line very close to which RRL/HB stars will spend most of their HB lifetimes. , compared with the observations (shaded bars).…”

Section: Theory Versus Observationsmentioning

confidence: 64%

“…We retrieved and employed the catalogs of RRL periods, photometric properties, and coordinates from 1 and Corwin & Carney (2001). These contain a total of more than 200 RRL stars with determined periods that can be used in our analysis.…”

Section: Discussionmentioning

confidence: 99%

“…Lowly reddened, relatively nearby, and having a long history of detailed observations, M3 was early noted to contain hundreds of RR Lyrae (RRL) variables, making it a ''splendid object for further studies'' (Bailey 1902). This, of course, was confirmed by all subsequent analyses (Bakos, Benkö, & Jurcsik 2000;Corwin & Carney 2001;Clement et al 2001 and references therein), which revealed that M3 is the GC with the largest (known) number of RRL variables, apart from ! Centauri (NGC 5139).…”

Section: Introductionmentioning

confidence: 88%

“…Inspection of the M3 CMD at the RRL region Corwin & Carney 2001) does reveal that the RRab region is much more densely populated than the RRc region. This is in sharp contrast with the canonical model predictions, in which the RRL strip is fairly uniformly populated from blue to red (Fig.…”

Section: Breakdown Of the Canonical Framework?mentioning

confidence: 99%

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The Evolutionary Status of M3 RR Lyrae Variable Stars: Breakdown of the Canonical Framework?

Catelan

2004

ApJ

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In order to test the prevailing paradigm of horizontal-branch (HB) stellar evolution, we use the large databases of measured RR Lyrae parameters for the globular cluster M3 (NGC 5272) recently provided by Bakos et al. and Corwin & Carney. We compare the observed distribution of fundamentalized periods against the predictions of synthetic HBs. The observed distribution shows a sharp peak at P f % 0:55 days, which is primarily due to the RRab variables, whereas the model predictions instead indicate that the distribution should be more uniform in P f , with a buildup of variables with shorter periods (P f < 0:5 days). Detailed statistical tests show, for the first time, that the observed and predicted distributions are incompatible with one another at a high significance level. This indicates either that canonical HB models are inappropriate, or that M3 is a pathological case that cannot be considered representative of the Oosterhoff type I (OoI) class. In this sense, we show that the OoI cluster with the next largest number of RR Lyrae variables, M5 (NGC 5904), presents a similar, although less dramatic, challenge to the models. We show that the sharp peak in the M3 period distribution receives a significant contribution from the Blazhko variables in the cluster. We also show that M15 (NGC 7078) and M68 (NGC 4590) show similar peaks in their P f distributions, which in spite of being located at a P f value similar to that of M3, can, however, be primarily ascribed to the RRc variables. Again similar to M3, a demise of RRc variables toward the blue edge of the instability strip is also identified in these two globulars. This is again in sharp contrast to the evolutionary scenario, which also foresees a strong buildup of RRc variables with short periods in OoII globulars. We speculate that in OoI systems RRab variables may somehow get ''trapped'' close to the transition line between RRab and RRc pulsators as they evolve to the blue in the H-R diagram, whereas in OoII systems it is the RRc variables that may get similarly trapped instead, as they evolve to the red, before changing their pulsation mode to RRab. Such a scenario is supported by the available CMDs and Bailey diagrams for M3, M15, and M68.

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Section: Theory Versus Observationsmentioning

confidence: 64%

Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 88%

Section: Breakdown Of the Canonical Framework?mentioning

confidence: 99%

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The Evolutionary Status of M3 RR Lyrae Variable Stars: Breakdown of the Canonical Framework?

Catelan

2004

ApJ

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“…For example, by adopting a mass range of M ¼ 0:65 0:80M , the expected dispersion in the reduced period, at constant A V , is D log P 0 F $ 0:09. Figure 7 shows the A V versus log P 0 F diagram for the Carina RRab stars, together with similar diagrams for variables in M3 (hV i m ¼ 15:62 mag; Corwin & Carney 2001) and M15 (hV i m ¼ 15:82 mag; Bingham et al 1984). We selected these two clusters because they host sizable samples of RR Lyrae stars (207 in M3, 88 in M15) for which accurate pulsation parameters are available, and they are the typical OoI (M3) and OoII (M15) Galactic prototypes.…”

Section: Identification Of Variablesmentioning

confidence: 90%

The Carina Project. I. Bright Variable Stars

et al. 2003

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We present new BV time series data of the Carina dwarf spheroidal galaxy (dSph). Current data cover an area of %0.3 deg 2 around the center of the galaxy and allow us to identify 92 variables. Among them 75 are RR Lyrae stars, 15 are bona fide anomalous Cepheids, one might be a Galactic field RR Lyrae star, and one is located along the Carina red giant branch. Expanding upon the seminal photographic investigation by Saha, Monet, & Seitzer we supply, for the first time, accurate estimates of their pulsation parameters (periods, amplitudes, mean magnitudes, and colors) on the basis of CCD photometry. Approximately 50% of both RR Lyrae stars and anomalous Cepheids are new identifications. Among the RR Lyrae sample, six objects are new candidate double-mode (RRd ) variables. On the basis of their pulsation properties we estimate that two variables (V158, V182) are about 50% more massive than typical RR Lyrae stars, while the bulk of the anomalous Cepheids are roughly a factor of 2 more massive than fundamental-mode (RRab) RR Lyrae stars. This finding supports the evidence that these objects are intermediate-mass stars during central He-burning phases. We adopted three different approaches to estimate the Carina distance modulus, namely, the first-overtone blue edge method, the period-luminosity-amplitude relation, and the periodluminosity-color relation. We found DM ¼ 20:19 AE 0:12, a result that agrees quite well with similar estimates based on different distance indicators. The data for Carina, together with data available in the literature, strongly support the conclusion that dSph's can barely be classified into the classical Oosterhoff dichotomy. The mean period of RRab's in Carina resembles that found for Oosterhoff type II clusters, whereas the ratio between first-overtone (RRc) pulsators and the total number of RR Lyrae stars is quite similar to that found in Oosterhoff type I clusters.

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2007

Nuclear Physics of Stars

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[ITAL]BV[/ITAL] Photometry of the RR Lyrae Variables of the Globular Cluster M3

Cited by 78 publications

References 38 publications

The Evolutionary Status of M3 RR Lyrae Variable Stars: Breakdown of the Canonical Framework?

The Evolutionary Status of M3 RR Lyrae Variable Stars: Breakdown of the Canonical Framework?

The Carina Project. I. Bright Variable Stars

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